A note on boundary value problems for black hole evolutions
| dc.creator | Dafermos, Mihalis | |
| dc.creator | Rodnianski, Igor | |
| dc.date | 2004-03-08 | |
| dc.date.accessioned | 2026-07-07T03:28:31Z | |
| dc.date.available | 2026-07-07T03:28:31Z | |
| dc.description | In recent work of Allen at. al., heuristic and numerical arguments were put forth to suggest that boundary value problems for black hole evolution, where an appropriate Sommerfeld radiation condition is imposed, would fail to produce Price law tails. The interest in this issue lies in its possible implications for numerical relativity, where black hole evolution is typically studied in terms of such boundary formulations. In this note, it is shown rigorously that indeed, Price law tails do not arise in this case, i.e. that Sommerfeld (and more general) radiation conditions lead to decay faster than any polynomial power. Our setting is the collapse of a spherically symmetric self-gravitating scalar field. We allow an additional gravitationally coupled Maxwell field. The proof also applies to the easier problem of a spherically symmetric solution of the wave equation on a Schwarzschild or Reissner-Nordstrom background. The method relies on previous work of the authors. | |
| dc.description | 8 pages, 3 figures | |
| dc.identifier | https://arxiv.org/abs/gr-qc/0403034 | |
| dc.identifier | http://arxiv.org/abs/gr-qc/0403034 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/34863 | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.title | A note on boundary value problems for black hole evolutions | |
| dc.type | text |